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dc.contributor.authorMatthews, Lynn D.
dc.contributor.authorGreenhill, Lincoln J.
dc.contributor.authorGoddi, C.
dc.contributor.authorChandler, C. J.
dc.contributor.authorHumphreys, E. M. L.
dc.contributor.authorKunz, M. W.
dc.date.accessioned2015-03-04T19:55:29Z
dc.date.available2015-03-04T19:55:29Z
dc.date.issued2010-01
dc.date.submitted2009-05
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://hdl.handle.net/1721.1/95819
dc.description.abstractWe present multi-epoch Very Long Baseline Array imaging of the [superscript 28]SiO v = 1 and v = 2, J = 1-0 maser emission toward the massive young stellar object (YSO) Orion Source I. Both SiO transitions were observed simultaneously with an angular resolution of ~0.5 mas (~0.2 AU for d = 414 pc) and a spectral resolution of ~0.2 km s[superscript –1]. Here we explore the global properties and kinematics of the emission through two 19-epoch animated movies spanning 21 months (from 2001 March 19 to 2002 December 10). These movies provide the most detailed view to date of the dynamics and temporal evolution of molecular material within ~20-100 AU of a massive (gsim8 M ☉) YSO. As in previous studies, we find that the bulk of the SiO masers surrounding Source I lie in an X-shaped locus; the emission in the south and east arms is predominantly blueshifted, and emission in the north and west is predominantly redshifted. In addition, bridges of intermediate-velocity emission are observed connecting the red and blue sides of the emission distribution. We have measured proper motions of over 1000 individual maser features and found that these motions are characterized by a combination of radially outward migrations along the four main maser-emitting arms and motions tangent to the intermediate-velocity bridges. We interpret the SiO masers as arising from a wide-angle bipolar wind emanating from a rotating, edge-on disk. The detection of maser features along extended, curved filaments suggests that magnetic fields may play a role in launching and/or shaping the wind. Our observations appear to support a picture in which stars with masses as high as at least 8 M ☉ form via disk-mediated accretion. However, we cannot yet rule out that the Source I disk may have been formed or altered following a recent close encounter.en_US
dc.description.sponsorshipNational Science Foundation (U.S.) (NSF grant 0507478)en_US
dc.description.sponsorshipSmithsonian Astrophysical Observatory (Visiting Scientist appointment)en_US
dc.language.isoen_US
dc.publisherInstitute of Physics/American Astronomical Societyen_US
dc.relation.isversionofhttp://dx.doi.org/10.1088/0004-637x/708/1/80en_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.sourceAmerican Astronomical Societyen_US
dc.titleA FEATURE MOVIE OF SiO EMISSION 20-100 AU FROM THE MASSIVE YOUNG STELLAR OBJECT ORION SOURCE Ien_US
dc.typeArticleen_US
dc.identifier.citationMatthews, L. D., L. J. Greenhill, C. Goddi, C. J. Chandler, E. M. L. Humphreys, and M. W. Kunz. “A FEATURE MOVIE OF SiO EMISSION 20-100 AU FROM THE MASSIVE YOUNG STELLAR OBJECT ORION SOURCE I.” The Astrophysical Journal 708, no. 1 (December 8, 2009): 80–92. © 2009 American Astronomical Society.en_US
dc.contributor.departmentHaystack Observatoryen_US
dc.contributor.departmentMIT Kavli Institute for Astrophysics and Space Researchen_US
dc.contributor.mitauthorMatthews, Lynn D.en_US
dc.contributor.mitauthorGreenhill, Lincoln J.en_US
dc.relation.journalAstrophysical Journalen_US
dc.eprint.versionFinal published versionen_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dspace.orderedauthorsMatthews, L. D.; Greenhill, L. J.; Goddi, C.; Chandler, C. J.; Humphreys, E. M. L.; Kunz, M. W.en_US
mit.licensePUBLISHER_POLICYen_US
mit.metadata.statusComplete


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